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Program 26 August — 20 September 2024
Understanding turbulent convection is of crucial importance in many fields of stellar astrophysics. For example, differential rotation and large-scale magnetic fields in stars owe their existence to turbulent convection. However, increasing evidence suggests that our understanding of stellar convection is much less complete than previously thought. The most dramatic manifestation of this is the wide discrepancy between the velocity amplitudes at large horizontal scales from helioseismic inferences and numerical simulations. We bring together experts in three-dimensional convection simulations, helio- and asteroseismology, theoreticians and observers present the latest developments and to address open problems in the field.
